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Detection of Scattered Light from the Hot Dust in HD 172555 ? ?? N

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Detection of Scattered Light from the Hot Dust in HD 172555 ? ?? N Astronomy & Astrophysics manuscript no. HD172555_v7_arxiv c ESO 2018 August 15, 2018 Detection of scattered light from the hot dust in HD 172555 ? ?? N. Engler1, H.M. Schmid1, S.P. Quanz1, H. Avenhaus2, and A. Bazzon1 1 ETH Zurich, Institute for Particle Physics and Astrophysics, Wolfgang-Pauli-Strasse 27, CH-8093 Zurich, Switzerland e-mail: [email protected] 2 Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany Received ...; accepted ... ABSTRACT Context. Debris disks or belts are important signposts for the presence of colliding planetesimals and, therefore, for ongoing planet formation and evolution processes in young planetary systems. Imaging of debris material at small separations from the star is very challenging but provides valuable insights into the spatial distribution of so-called hot dust produced by solid bodies located in or near the habitable zone. We report the first detection of scattered light from the hot dust around the nearby (d = 28:33 pc) A star HD 172555. Aims. We want to constrain the geometric structure of the detected debris disk using polarimetric differential imaging (PDI) with a spatial resolution of 25 mas and an inner working angle of about 0.100. Methods. We measured the polarized light of HD 172555, with SPHERE-ZIMPOL, in the very broad band (VBB) or RI filter 00 00 (λc = 735 nm, ∆λ = 290 nm) for the projected separations between 0:08 (2.3 au) and 0:77 (22 au). We constrained the disk parameters by fitting models for scattering of an optically thin dust disk taking the limited spatial resolution and coronagraphic attenuation of our data into account. Results. The geometric structure of the disk in polarized light shows roughly the same orientation and outer extent as obtained from thermal emission at 18 µm. Our image indicates the presence of a strongly inclined (i ≈ 103:5◦), roughly axisymmetric dust belt with an outer radius in the range between 0.300 (8.5 au) and 0.400 (11.3 au). An inner disk edge is not detected in the −5 data. We derive a lower limit for the polarized flux contrast ratio for the disk of (Fpol)disk=F∗ > (6:2±0:6)·10 in the VBB filter. This ratio is small, only ∼9 %, when compared to the fractional infrared flux excess (≈ 7:2 · 10−4). The model simulations show that more polarized light could be produced by the dust located inside ≈ 2 au, which cannot be detected with the instrument configuration used. Conclusions. Our data confirm previous infrared imaging and provide a higher resolution map of the system, which could be further improved with future observations. Key words. Planetary systems – Scattering – Stars: individual object: HD 172555, HR 7012, HIP 92024 – Techniques: high angular resolution, polarimetric 1. Introduction (e.g., Moerchen et al. 2010; Schneider et al. 2014; Choquet et al. 2016; Olofsson et al. 2016; Bonnefoy et al. 2017). Young stars are often surrounded by circumstellar dust debris disks or rings. These consist of solid bodies, such as planetes- In the absence of imaging data, the location of the bulk of imals and comets, as well as large amounts of dust and small dust in the system can be inferred from the grain temperature amounts of gas. Small dust grains with a broad size distribu- derived by SED modeling. Based on modeling results, most tion are generated in steady collisions of solid bodies and per- debris disks have been found to harbor warm dust, meaning haps by the evaporation of comets. Debris disks are usually that the temperature of small grains lies between 100 and recognized by infrared (IR) excess on top of the spectral en- approximately 300 K (e.g., Moór et al. 2006; Trilling et al. ergy distribution (SED) of the stellar photosphere because of 2008; Chen et al. 2011; Morales et al. 2011). Cold debris the thermal emission of the heated dust grains (see, e.g., Wyatt reside far away from the host star where their temperature 2008; Matthews et al. 2014, for a review). In scattered light, does not exceed 100 K. The prominent analogs to warm and debris disks are usually very faint, i.e., > 103 times fainter cold dust belts are the main asteroid belt at 2-3.5 au and the arXiv:1808.04373v1 [astro-ph.EP] 13 Aug 2018 than the host star, and therefore they are difficult to image. To Kuiper belt between 30 and 48 au in the solar system (Wy- date, several dozen debris disks have been spatially resolved att 2008). Aside from this, several stars with hot disks have in various wavelength bands, from visible to millimeter, using been found (Wyatt et al. 2007a; Fujiwara et al. 2009) based various space and ground-based telescopes. These data pro- on the IR excess with an estimate temperature above 300 K. vide important constraints on the debris disk morphologies The stars that possess hot dust are very interesting targets be- cause the submicron-sized grains at a small small distance ? Based on data collected at the European Southern Observatory, from a star could be a signpost for transient collision events. Chile under program 095.C-192 HD 172555 (HIP 92024, HR 7012) is one of the most stud- ?? The reduced images as FITS files are available in electronic form ied objects among these special stellar systems (Cote 1987; at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) Schütz et al. 2005; Chen et al. 2006; Wyatt et al. 2007b; Lisse or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/ et al. 2009; Smith et al. 2012; Riviere-Marichalar et al. 2012; Article number, page 1 of 16 A&A proofs: manuscript no. HD172555_v7_arxiv Johnson et al. 2012; Kiefer et al. 2014; Wilson et al. 2016; 2. Observations Grady et al. 2018). Observations of HD 172555 were taken in service or queue HD 172555 is a V = 4.8m, A7V star (Høg et al. 2000; Gray mode during six runs in 2015 as part of the open time pro- et al. 2006) at a distance of 28:33 ± 0:19 pc (Gaia Collabo- gram 095.C-192 using ZIMPOL, the visual subsystem of the ration 2016) and a member of the β Pictoris moving group. SPHERE (Spectro-Polarimetric High-contrast Exoplanet RE- The deduced age for the group is 23 ± 3 Myr (Mamajek & search) instrument. The SPHERE instrument was developed Bell 2014). HD 172555 has a K5Ve low mass companion for high contrast observations in the visual and near-IR spec- 00 CD-64 1208, separated by more than 2000 au or 71.4 (Tor- tral range and includes an extreme adaptive optics (AO) sys- res et al. 2006). The Infrared Astronomical Satellite (IRAS) tem and three focal plane instruments for differential imaging identified HD 172555 as a Vega-like star that has a large IR (Beuzit et al. 2008; Kasper et al. 2012; Dohlen et al. 2006; excess with an effective temperature of 290 K (Cote 1987). Fusco et al. 2014, Schmid et al. 2018, submitted). Mid-infrared (mid-IR) spectroscopy from the ground (Schütz et al. 2005) and 5.5-35 µm spectroscopy obtained with the The ZIMPOL polarimetry is based on a modulation- Spitzer Infrared Spectrograph (IRS) show very pronounced demodulation technique and our observations of HD 172555 SiO features (Chen et al. 2006, their Fig. 2(d)) indicating in the VBB filter were carried out in the fast modulation large amounts of submicron sized crystalline silicate grains mode using field stabilization, which is also known as the with high temperatures (> 300 K). Lisse et al. (2009) pro- P2 derotator mode. The ZIMPOL modulation technique mea- posed, based on the spectral analysis of mineral features, that sures the opposite polarization states of incoming light quasi- the IR-excess emission originates from a giant collision of simultaneously and with the same pixels such that differential large rocky planetesimals similar to the event that could have aberrations between I? and Ik are minimized. Fast modulation created the Earth-Moon system. means a polarimetric cycle frequency of 967.5 Hz, which is obtained with a ferro-electric liquid crystal (FLC) and a polar- Until now, only one resolved image of the HD 172555 ization beam splitter in front of the demodulating CCD detec- − debris disk existed that was obtained in the Qa band (λc = tor. The high detector gain of 10.5 e /ADU allows broadband 18:30 µm, ∆λ = 1:52 µm; hereafter Q band) with TReCS observations with high photon rates without pixel saturation (Thermal-Region Camera Spectrograph) at Gemini South and ensures high sensitivity at small angular separations at the telescope and described by Smith et al. (2012). They detected expense of a relative high readout noise. The ZIMPOL VBB extended emission after subtraction of a standard star point or RI filter used (λc = 735 nm, ∆λ = 290 nm) covers the spread function (PSF), which is consistent with an inclined R band and I band. Polarimetric data were taken in corona- disk with an orientation of the major axis of θ = 120◦, an graphic mode using the Lyot coronagraph V_CLC_MT_WF inclination of ≈ 75◦, and a disk outer radius of 8 au. In Si-5 with a diameter of 155 mas. The mask is semi-transparent filter (λc = 11:66 µm, ∆λ = 1:13 µm; hereafter N band) data, such that the central star is visible as faint PSF in the mid- the disk was not detected. Combining these results with the dle of attenuation region if the stellar PSF is of good quality visibility functions measured with the MID-infrared Interfer- (good AO corrections) and well centered on the mask.
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